This article was accepted into the corpus but its outbound wikilinks were never NER-processed — typical at the deepest BFS hop or when the run's entity cap was reached. No expansion funnel to show.
| Castelli & Kurucz | |
|---|---|
| Name | Castelli & Kurucz |
| Occupation | Astronomical modelers |
| Known for | Stellar atmosphere models and synthetic spectra |
| Notable works | ATLAS models, opacity distribution functions, synthetic spectra grids |
Castelli & Kurucz
Castelli & Kurucz contributed extensive stellar atmosphere models used across observational programs such as Hubble Space Telescope, Gaia (spacecraft), Sloan Digital Sky Survey, Kepler (spacecraft), TESS and research groups at institutions like Harvard–Smithsonian Center for Astrophysics, Max Planck Institute for Astronomy, European Southern Observatory, Institute of Astronomy, Cambridge, and Carnegie Observatories. Their work builds on theoretical foundations from researchers associated with R. L. Kurucz, F. Castelli, David L. Lambert, Gustafsson Carl, Martin Asplund, Paul Barklem, Anil Pradhan and software environments used at NASA, National Optical Astronomy Observatory, Space Telescope Science Institute, European Space Agency, and Smithsonian Astrophysical Observatory.
The models provide plane-parallel, one-dimensional grids widely used alongside grids from PHOENIX (program), MARCS (model atmospheres), CMFGEN, TLUSTY and Kurucz models in analyses for stellar parameters of targets from surveys like RAVE, LAMOST, GALAH, APOGEE and missions such as Hipparcos. Grids span effective temperatures, surface gravities and compositions relevant to stars observed in programs at observatories including Keck Observatory, Very Large Telescope, Subaru Telescope, Gemini Observatory and datasets from 2MASS, WISE, Pan-STARRS.
The approach incorporates opacity sources and line lists developed in collaboration with projects and databases such as VALD, Kurucz line lists, NIST Atomic Spectra Database, Opacity Project, IRON Project and theoretical work by groups at University of Chicago, California Institute of Technology, Princeton University and University of Cambridge. Treatment of continuum and line opacities relates to studies by Gustafsson Carl, Hubeny Ivan, Kurucz Robert, Seaton Michael, Berrington Keith, Hummer Derek, and methods applied in codes used at Los Alamos National Laboratory and Lawrence Livermore National Laboratory.
Researchers apply the models to abundance analyses associated with stars in clusters like M13 (globular cluster), M92, Omega Centauri, Hyades, Pleiades (star cluster), and to stellar populations in galaxies such as Milky Way, Andromeda Galaxy, Large Magellanic Cloud, Small Magellanic Cloud, and surveys by teams at Max Planck Institute for Astrophysics, Institute for Advanced Study, University of California, Berkeley, University of Cambridge, University of Michigan. Applications include spectral fitting for programs linked to VLT-FLAMES, HIRES, UVES, APOGEE spectrograph and comparison with theoretical yields from groups like Woosley & Weaver, Nomoto, Kobayashi (astrophysicist).
Comparisons contrast assumptions with models from PHOENIX (program), MARCS (model atmospheres), TLUSTY, ATLAS9, ATLAS12 and non-LTE codes such as CMFGEN and MULTI (code), and with empirical calibrations tied to standards like Vega, Arcturus, Sirius, Procyon. Studies by teams at Stockholm University, University of Uppsala, University of Tokyo and Monash University evaluate differences in line formation, convection treatment and molecule formation when comparing to datasets from HERMES spectrograph, GALAH survey and archives at European Southern Observatory.
Revisions incorporated updated opacities, line lists and microphysics inspired by work from R. L. Kurucz, F. Castelli, Martin Asplund, Paul Barklem, Maria Bergemann and collaborations involving National Science Foundation, European Research Council, Royal Society funding for projects at University of Chicago, Observatoire de Paris, Max Planck Institute for Astrophysics and software improvements paralleled advances in computing at Lawrence Berkeley National Laboratory, Advanced Research Computing centers and supercomputing facilities used by NASA Advanced Supercomputing.
The models influenced pipelines and analysis frameworks used by teams at Sloan Digital Sky Survey, Gaia-ESO Survey, APOGEE, GALAH survey and observatories including Keck Observatory, European Southern Observatory, Magellan Telescopes; they shaped stellar parameter scales and abundance patterns interpreted in studies by Freeman Ken, Bland-Hawthorn Joss, Helmi Amina, Majewski Steven, Rix Hans-Walter and informed chemical evolution models from groups such as Prantzos', Chiappini, Matteucci. Their legacy persists in spectral synthesis tools and community databases maintained by CDS (Centre de Données astronomiques de Strasbourg), SIMBAD, VizieR and continues to support research at institutions including Harvard University, University of Cambridge, Max Planck Institute for Astronomy and Space Telescope Science Institute.
Category:Stellar atmosphere models